Kβ Satellite Research Articles

Theoretical calculation of Kα and Kβ X-ray satellite and hypersatellite structures for hollow argon atoms

A systematical knowledge of the satellite and hypersatellite structures of X-ray transitions is of great interest for various research areas, such as the explanation of the X-ray radiation from universe, plasma diagnostics, extreme ultraviolet (EUV) and X-ray sources and so on. Among these researches, the detailed explanation of the complex structures of X-ray satellites and hypersatellites are crucial for understanding the X-ray emission mechanism and the hollow atom formation mechanism. In this paper, the Kα and Kβ X-ray satellite and hypersatellite structure are theoretically studied for hollow argon atoms with the relativistic multiconfiguration Dirac-Fock (MCDF) method, which includes the Breit and quantum electro-dynamics (QED) corrections. To check the applicability of the method, the transition energies and rates of the diagram lines for Ar are calculated,. and the results are in agreement with previously published data. Then the MCDF calculations of the transition energies and probabilities of Kα 1, 2 (K →L3, 2) and Kβ 1, 3 (K → M3, 2) X-ray satellites and hypersatellites, which originate from the argon atoms with additional vacancies in the L shell, are carried out. To obtain the overall profile of the K X-ray spectrum, the diagram lines are integrated with the satellites and hypersatellites on the assumption that the intensity is proportional to the corresponding transition probability and each discrete line has a Gaussian distribution profile with a full width at half maximum (FWHM) value of 20 eV. From the convoluted profile, we can obtain the dependence of the average transition energy and relative transition intensity of the satellites and hypersatellites on the initial hollow configuration. It is found that the transition energy shift increases linearly with the number of spectator vacancies in the L shell increasing. For instance, the energy shift of the Kα satellite caused by L-shell hole is about 20 eV, and that of the Kβ satellite is 48 eV. While for hypersatellite, the energy shift increases greatly due to the double ionization in the K shell. The energy shift increment of Kα and Kβ hypersatellites corresponding to L vacancy are 21 and 52 eV, respectively. Finally, four simple empirical formulae for estimating the energy shifts of the Kα, Kβ X-ray satellites and hypersatellite for Ar atom with any number of L-shells vacancies are deduced by using the least square method. These results are useful in explaining various K X-ray spectra and better understanding the collision process.

Energy shifts of Kα,β,γ X-ray satellites for atoms with 13 ⩽ Z ⩽ 90: A systematic calculation and a new analytical description

The transition energy shifts of the Kα, Kβ and Kγ X-rays resulted from addition vacancies in L-shell for atoms with 13⩽Z⩽90 have been calculated systematically, by using the Flexible Atomic Code (FAC), in which the Breit interaction, QED corrections and nuclear finite mass effects are also considered. It is shown by means of concrete figures that the overall agreement among the present results, theoretical results of other authors as well as a large body of measured ones was excellent. Contrary to other discussions, we found that the energy shifts of the Kα and Kβ satellites did not varies absolutely linearly with Z, the contributions of the Z2 term cannot be neglected, and the energy differences between neighboring L satellites were not equal. Three simple empirical formulae for estimating the energy shifts of the Kα, Kβ and Kγ X-ray satellites for any atom with any number of L-shell vacancies were put forward. They will be useful in qualitative interpretation of various K X-ray spectra and better understanding of the collision processes.

X-ray Fluorescence Analysis of Hexavalent Chromium Using Kβ Satellite Peak Observed as Counterpart of X-ray Absorption Near-Edge Structure Pre-Edge Peak

A Kβ satellite peak in X-ray fluorescence (XRF) spectra is observed as a counterpart of the pre-edge peak of the X-ray absorption near edge structure (XANES). In Kβ emission of chromium, a small satellite peak is observed at 5.983-5.988 keV only for hexavalent chromium compounds such as CrO(3), Na(2)CrO(7)·2H(2)O, Na(2)CrO(4)·4H(2)O, K(2)Cr(2)O(7), K(2)CrO(4), Zn(2)CrO(4)(OH)(2)·2H(2)O, PbCrO(4), and BaCrO(4), together with the main peak at 5.947 keV, while trivalent chromium compounds such as Cr(2)O(3) and Cr(OH)(3)·nH(2)O show only the main peak at 5.947 keV. This corresponds to the fact that the K pre-edge peak in XANES is observed only for the hexavalent chromium compounds. The electronic level causing the satellite peak is almost at the same energy level as that causing the pre-edge peak. Our finding not only affects the interpretation of the origin of the pre-edge peaks but also leads to the simple speciation method of chromium compounds using XRF.

Elucidation of the chemical state of phosphorus and boron in crystallographically amorphous nickel electroplates

Using the valence-to-core version of X-ray emission spectroscopy (valence-to-core XES) together with X-ray diffraction analysis, the structure and the composition of nickel coatings deposited from solutions containing hypophosphite ions or dimethylaminoborane (DMAB) are studied. The diffraction patterns of prepared deposits are characterized by the presence of a wide “halo”. Annealing of crystallographically amorphous deposits at temperatures of 500°C and higher transforms these haloes into the spectra corresponding to metal nickel and its phosphides or borides present in the crystallized deposits. A result of fundamental importance obtained in the simultaneously conducted examination of the same deposits by the valence-to-core XES method is that both the binding energy and the intensities of Kβ satellite spectral lines of annealed samples remain unchanged as compared with original samples. Based on this comparison, it is concluded that phosphide and boride nickel compounds were already formed in the course of electrodeposition, whereas the thermal treatment of deposits (crystallization) leads only to aggregation of the metal and metal-metalloid nanoparticles.

Kα and Kβ satellite and hypersatellite fluorescence yields of Mg and Si

Decay schemes of Mg and Si atoms, in all possible vacancy configurations that decay via K X-ray emission, were studied to determine the correspondence (fluorescence yields) of Kα and Kβ photon yields to the initial state production yields. The K shell fluorescence yields and non-radiative decay rates of singly ionized atoms, were taken from literature, while non-radiative decay rates of multiply ionized atoms were determined using the Larkins approach.The correspondence of photon yields to the initial state production yields was written in a matrix form. The matrix was used also to determine relative yields of components contributing to single Kα satellites or hypersatellites, and Kβ photon yields from Kα photon yields. These values are crucial to analyze properly the Kα hypersatellite region where there is an overlap with the Kβ satellites. In the Kα satellite region, where there is no overlap, the relative yields can be used for the evaluation of the modeled lineshapes. The calculated values were evaluated on measured spectra and were found to be satisfactory.

Configurations of highly ionized fast sulphurprojectiles passing through a carbon foil evaluated fromlow-resolution K x-ray spectra

The Kα and Kβ satellite and hypersatellite x-raylines for highly ionized sulphur projectiles passing throughcarbon foils of thickness between 15-210 µg cm-2with energies of 99 and 122 MeV have been recorded using aSi(Li) detector. A new theoretical model based on the resultsof single-configuration Dirac-Fock calculations (and usingequilibrium charge state distribution and fluorescence yields)has been proposed in order to evaluate the average populationof different shells and to estimate the probability ofappearance of the most important configurations in the sulphurions passing through the carbon foils. The reliability of themodel has been proved by a very good reproduction of themeasured energy shifts for all Kα and Kβ satelliteand hypersatellite peaks. The role of non-equilibrium chargefractions in various shells of sulphur ions has also beeninvestigated in detail.

Target-atom inner-shell vacancy distributions created in collisions with heavy ion projectiles

A model of the evolution of Cu atom inner-shell electron configurations was developed in order to establish the relationship between the original populations created in K-vacancy producing collisions with fast heavy-ion projectiles and those that exist at the time of Cu Kα and Kβ X-ray emission. The model takes into account multi-step vacancy rearrangement processes that may occur prior to K X-ray emission. An iterative procedure is employed in which a set of trial parameters that define the original inner-shell population distributions are varied to obtain satisfactory agreement of the calculated Kα satellite relative intensities and energies, as well as the overall intensity ratio of Kβ satellites to Kα satellites, with the experimental data. In addition to deducing the properties of the original L- and M-shell population distribution, this procedure also provides the average value of the fluorescence yield for conversion between X-ray and K-vacancy production cross sections.

Energy calculation of K 1L 1 multiply ionized Kβ satellite spectra emitted from Al, Al 2O 3, Si and SiO 2

Final states of a Kβ X-ray transition from a K 1L 1 multiply ionized state and a KLV Auger transition from a K 1L 0 state are common in electronic configurations. Considering the above situation we developed a new method to calculate energies of the Kβ satellites emitted from the third-row elements in which informations on chemical bondings are reflected. For this purpose observed energies of the KLV Auger and calculated results for isolated atoms using the nonrelativistic Hartree-Fock-Slater orbital calculation were employed. The energies of the K 1L 1 Kβ satellites which were emitted from Al, Al 2O 3, Si and SiO 2 were calculated here for the first time.

Kβ satellite spectrum of metallic nickel

The electron excited Kβ emission spectrum of metallic nickel has been recorded photographically by a 40 cm curved muscovite mica spectrograph of the Cauchois type, and analysed by a microphoometer. Both high and low energy sides of the Kβ 1.3 line have been studied in detail. On the high energy side, a new satellite at 1492.7 xu (8288.5 eV) has been observed and has been named as β 7. The presence of the satellites ξ III, ξ IV and β IV 1 reported earlier, each in only one study, has been confirmed. The last line has been renamed as β 6. Many of the other satellites, reported earlier, have been remeasured. The transition assignments to these satellites, based on HFS calculations of 1s(−1) nl(− m)− nl(− m)3p(−1); n = 2, 3; m = 1, 2; transition energies, have been presented. On the low energy side of the Kβ 1.3 line, many new features have been observed. The presence of the satellites β η and β q, reported earlier, has been confirmed. It has been reported that many of these low energy satellites can be assigned to various 1 s(−1)−3l,(−1)3l,( t ̄ 1) , ( l i = 0, 1; l i = 0, 1 and 2) radiative Auger transition.

X-ray fluorescence analysis of the concentration and valence state of sulfur in pollution samples

Two special X-ray spectrometers have been developed for the measurement of sulfur pollution. One of them is a portable instrument which uses a 50 W aircooled X-ray tube and a vacuum spectrometer with a NaCl crystal. It can detect 0.5μg/cm 2 of S in 100-s counting interval. The other instrument is specifically for the measurement of valence state of sulfur. It consists of a replacement channel for the multiple-crystal spectrometer instrument used by the Environmental Protection Agency for routine analysis. With this replacement channel details of the sulfur spectrum can be scanned or the crystal may be set for the sulfate Kβ satellite for routine determination of the sulfate fraction of total sulfur.

The Kα and Kβ X-ray spectra of Al, Ti, Cr, Fe and Ni induced by 84 MeV nitrogen ions

The K X-rays from the target elements due to N-ion bombardment are measured with a crystal spectrometer. Some aspects owing to high incident energy are discussed. The Kα satellite, Kα hypersatellite and Kβ satellite peak spacings are obtained.

Kβ Satellites in Fluorescence Spectra of Some Mg and Al Compounds

The high energy Kβ satellites βIII, βIV, βVII, βVII have been studied in fluorescence. Their in­tensities have been correctd for the self-absorption effect by measuring the intensities from Mg and A1 compounds having various absorption coefficients. By comparing the energy and intensity of the βIII βIV group with the calculations of the sudden approximation theory we have shown that this group is due to double-hole states. It is proposed that the α10 α11 group on the low energy side of the Kβ line arises from transitions between quadri-hole states. The line usually designated as Kβ' is thought to arise from a cross transition between the cation and anion in Mg, Al, and Si compounds involving the second period elements.

Some investigations in Röntgen spectra. Part I.─X-ray spark lines

As is now well known there are certain lines in Röntgen spectra which cannot be fitted up into the usual energy level diagram even after violating the selection rules ∆ j = ± 1, 0, and ∆1 = ±1. These are called “non-diagram” lines or “spark” lines although the latter designation is somewhat anomalous in as much as the usual diagram lines are, regularly, lines due to transitions in an atom deprived of one of the electrons of the completed groups. They are found on the short as well as on the long wave-length side of the principal diagram lines, and consequently it has been customary to describe them as “satellites” of the principal lines. After their first discovery by Siegbahn and Stenström their number has rapidly grown large. Recently Beuthe has measured the β‴ line for elements V (23) to Y (39) and has also discovered a new line η for some of these elements. The problem of X-ray spark lines is little understood, and it is desirable to study closely the satellites of the principal lines for many elements in the several series. As a first step towards the achievement of this end a close study of Kα and Kβ satellites of the elements Si (14) to Cl (17) was undertaken. The results obtained go to show that the structure of the satellites is complex and that their nature is highly dependent upon the state of chemical combination of the atom which emits them.